Context. Galactic cosmic rays are widely assumed to arise from diffusive shock acceleration, specifically at shocks in supernova remnants (SNRs). These shocks expand in a complex environment, particularly in the core-collapse scenario as these SNRs evolve inside the wind-blown bubbles created by their progenitor stars. The cosmic rays (CRs) at core-collapse SNRs may carry spectral signatures of that complexity. Aims. We study particle acceleration in the core-collapse SNR of a progenitor with initial mass 60 $M_\odot$ and realistic stellar evolution. The SNR shock interacts with discontinuities inside the wind-blown bubble and generates several transmitted and reflected shocks. We analyse their impact on particle spectra and the resulting emission from the remnant. Methods. The hydrodynamic equations for the evolution of SNR inside the pre-supernova circumstellar medium have been solved simultaneously with the transport equation for cosmic rays in test-particle approximation and with the induction equation for the magnetohydrodynamics (MHD) in 1-D spherical symmetry. Results. The evolution of core-collapse SNRs inside complex wind-blown bubbles modifies the spectra of both the particles and their emission. We have found softer particle spectra with spectral indices close to 2.5 during shock propagation inside the shocked wind, and this softness persists at later evolutionary stages. Further, our calculated total production spectrum released into the interstellar medium demonstrates spectral consistency at high energy with the galactic CRs injection spectrum, required in propagation models. The magnetic field structure effectively influences the emission morphology of SNR as it governs the transportation of particles and the synchrotron emissivity.
The impact of circumstellar wind-blown bubbles on the dynamics of pulsar wind nebulae and supernova remnants
Gran Sasso Science Institute (GSSI)（格兰萨索科学研究所）；INFN-Laboratori Nazionali del Gran Sasso (LNGS)（意大利国家核物理研究院格兰萨索国家实验室）；IRAP, Université de Toulouse, CNRS, CNES（图卢兹大学、法国国家科学研究中心、法国国家空间研究中心天文物理研究）
We report on CO and HI studies of the mixed-morphology supernova remnant (SNR) G346.6$-$0.2. We find a wind-blown bubble along the radio continuum shell with an expansion velocity of $\sim10$ km s$^{-1}$, which was likely formed by strong stellar winds from the high-mass progenitor of the SNR. The radial velocities of the CO/HI bubbles at $V_\mathrm{LSR} = -82$-$-59$ km s$^{-1}$ are also consistent with those of shock-excited 1720 MHz OH masers. The molecular cloud in the northeastern shell shows a high-kinetic temperature of $\sim60$ K, suggesting that shock-heating occurred. The HI absorptio…
Expanding molecular bubble surrounding Tycho's supernova remnant (SN 1572) observed with IRAM 30 m telescope: evidence for a single-degenerate progenitor
Ia超新星的前身是单简并还是双简并白矮星系统一直是一个备受争议的话题。为了解决Ia型第谷超新星遗迹（SNR）SN 1572的起源，我们进行了$^{12}$ CO J=2-1映射和使用IRAM 30米望远镜对遗迹进行3毫米线测量。我们表明，第谷是包围着一个clusterous分子泡在当地的标准的$\sim 61$公里的$^{-1}$的速度为$\sim 4.5$公里的$^{-1}$，并有一个质量为$\sim 220$ M $_\odot$（在距离为2.5千秒差距）。增强的$^{12}$ CO J=2-1线发射相对于$^{12}$ CO J=1-0发射和可能的线加宽（在速度范围$-64$到$-60$ km s $^{-1}$）被发现在东北边界的SNR，在那里的壳变形和减速。这些功能，结合膨胀的分子泡和第谷之间的形态对应关系，表明SNR是与泡沫在速度范围$-66$到$-57$ km s $^{-1}$。最合理的起源膨胀的泡沫是快速流出（速度为数百公里秒$^{-1}$）驱动的WD附近，因为它吸积的物质从一个非退化的伴星。在低密度风吹气泡中，信噪比一直在扩大，冲击波刚刚到达分子腔壁。在低密度风吹气泡中，信噪比一直在扩大，冲击波刚刚到达分子腔壁。这是第一次明确检测到Ia型SNR的祖先驱动的膨胀气泡，这构成了Ia型SN的单一简并祖先的证据。
Probing hadronic gamma-ray and high-energy neutrino emission from Gaia DR2 star clusters
Friedrich-Alexander-Universität Erlangen-Nürnberg（埃尔朗根-纽伦堡大学）；Istituto Nazionale di Astrofisica, Osservatorio Astrofisico di Arcetri（国家天体物理研究所，阿切特里天文台）；Sapienza Università di Roma（罗马智慧大学）；Istituto Nazionale di Fisica Nucleare, Sezione di Roma（国家核物理研究所，罗马分部）；Instituto de Astrofìsica de Andalucìa, CSIC（安达卢西亚天体物理学研究所，西班牙高等科学研究理事会）；Erlangen Centre for Astroparticle Physics（埃尔朗根高能粒子物理中心）
We probe the environmental properties of X-ray supernova remnants (SNRs) at various points along their evolutionary journey, especially the S-T phase, and their conformance with theoretically derived models of SNR evolution. The remnant size is used as a proxy for the age of the remnant. Our data set includes 34 Milky Way, 59 Large Magellanic Cloud (LMC), and 5 Small Magellanic Cloud (SMC) SNRs. We select remnants that have been definitively typed as either core-collapse (CC) or Type Ia supernovae, with well-defined size estimates, and a thermal X-ray flux measured over the entire remnant. A c…
We report new HI observations of the Type Ia supernova remnant SN 1006 using the Australia Telescope Compact Array with an angular resolution of $4.5' \times 1.4'$ ($\sim$2 pc at the assumed SNR distance of 2.2 kpc). We find an expanding gas motion in position-velocity diagrams of HI with an expansion velocity of $\sim$4 km s$^{-1}$ and a mass of $\sim$1000 $M_\odot$. The spatial extent of the expanding shell is roughly the same as that of SN 1006. We here propose a hypothesis that SN 1006 exploded inside the wind-blown bubble formed by accretion winds from the progenitor system consisting of …
A high resolution HI study towards the supernova remnant Puppis A and its environments
我们观察超新星遗迹（SNR）船尾座A在21厘米线与澳大利亚望远镜紧凑阵列的目的是确定系统的速度，因此，相应的运动学距离。对于紧凑的，在现场的背景源，我们得到的吸收光谱，通过应用两种方法：（a）减去轮廓上和关闭源连续发射，和（b）过滤傅立叶平面中的短空间频率，以消除大规模的发射。船尾座A外壳东部最亮的特征之一被发现是背景源，可能是河外星系。除去这个和以前已知的不相关的源的贡献，船尾座A的系统速度被限制在8和12 km s $^{-1}$之间，这使得这个源的距离为1.3 $\pm$ 0.3 kpc。从包括单碟和干涉数据的组合图像中，我们分析了星际氢的分布。我们认为，如果距离为$\lesssim$ 1.2 kpc，那么在$v \sim $ +8 km s $^{-1}$处的椭球环可能是船尾座A的祖先吹出的气泡的遗迹。与以前的出版物（$v =$ +16 km s $^{-1}$和$d = $ 2.2 kpc）相比，新的系统速度和距离的主要结果是在东方没有一个致密的相互作用云来解释形态，以及壳层尺寸和中子星速度的减小，现在与统计值更好地吻合。
